adsabs/AstroCLIMB huggingface dataset:
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The fraction of class “B” photons as a function of energy for each case of simulation. The area enclosed under each curve is normalized to unity. In our simulation, the radiation of AC is totally fan beamed; if there is some pencil beamed AC radiation, the spectra of class “B” photons will be softer.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The observed total flux of classes “A” and “B” photons at different observing inclination angles averaged over all azimuth angles around the z-axis.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Collimation factor as a function of observing inclination angle averaged over all azimuth angles around the z-axis.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The fraction of class “B” photons as a function of observing inclination angle for each case of simulation. The area enclosed under each curve is normalized to unity.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Distribution functions of ﹩\mathrm{log}({e}_{H})﹩ for the Hi-GAL W3 250 μm image. These are displayed vertically at different coverages N  B  arranged along the x-axis. The predicted locus based on a common s  i  passes through the peak for each coverage. The long tails to high e  H  are modeled by including a second gradient-related component parameterized by s  g  (Section 5).
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Dispersion of the 250 μm JDM of W3 (green dots) for pixels in bins of increasing predicted dispersion from instrument noise and gradient-related noise. Left and right panels are for native maps and those convolved to 500 μm resolution, respectively. Red and blue curves show the contributions of instrument noise and gradient-related noise to the JDM dispersion for pixels in a bin, which added in quadrature give the one-to-one gray lines. For the same bins, a revised prediction of the JDM dispersion (purple) includes a constant contribution, added in quadrature, from low spatial frequency undulations (orange), which is most reliably quantified in the convolved map, as in companion Figure 6.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: 2D histogram showing correlation of Herschel 160 μm map of the Perseus E field with that from the Planck thermal dust model. Top maps: Planck model and HSA PACS 160 μm map convolved to Planck resolution and adjusted to Planck using the correlation line, respectively. Bottom maps: fractional-residual map of model minus adjusted HSA map, and residual of the same two maps. The white holes in all four maps show the masked pixels (see text).
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Like Figure 11 but for 250 μm. Here the zero-level adjustment is close to zero because the HSA SPIRE 250 μm map had already been adjusted by 47.69 MJy sr−1.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Dispersion of the 250 μm JDM of W3 (green dots) for pixels in bins of increasing predicted dispersion from instrument noise, on the right for native maps and on the left for maps convolved to 500 μm resolution. Red one-to-one lines show the contributions of instrument noise to the JDM dispersion for pixels in a bin. For the same bins, a revised prediction of the JDM dispersion (purple) includes a constant contribution, added in quadrature, from low spatial frequency undulations (orange), which is most reliably quantified in the convolved map. This figure is a companion of the low-x ends of Figure 7 in Section 5.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Distribution function of ﹩\mathrm{log}({e}_{H})﹩ from Figure 4, at coverage N  B  = 10. Red curve is the model for pixels with small gradients (dark shaded histogram), dominated by instrument noise based on s  i . Blue curve is for the unmasked ensemble, which depends on both s  i  and s  g  for errors added in quadrature (see text).
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: 2D histograms of gradient-scaled uncertainty with respect to intensity-scaled uncertainty at 250 μm. The one-to-one line is shown in pink. The black circle represents the median common uncertainty. Top: for the Perseus E field. Bottom: for the Tau T3 field in the Taurus molecular cloud complex.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: 2D histograms of total uncertainty (MJy sr−1) at passband 160, 350, and 500 μm with respect to 250 μm. The pink line is simulated fit based on simplified assumptions that are explained in Section 8.4. The dotted black line is simply a one-to-one line.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Distribution of the median of the intensity-scaled uncertainties for all fields (MJy sr−1). Vertical solid black line represents the common uncertainty for each passband, whereas the vertical black and red dotted lines are for Perseus E and Tau T3, respectively.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: The sky distribution of all LAEs (white open circles) in the context of Hyperion. The extent of Hyperion reported by Cucciati et al. (2018) is shown in the top left panel as a black dashed line with the known spectroscopic members marked as triangles. The color contours represent the seven density peaks of Hyperion color-coded by their redshifts, of which the four largest protocluster members are those reported by Ch15 and D16 (top right), D16 (bottom left), and W16 (bottom right). The redshift range of these individual protoclusters and their number of spectroscopic sources are found at the top of each panel; these galaxies are plotted as squares. The smoothed LAE density maps in the background are identical to that shown in the top left panel of Figure 4. The region covered by VUDS and HPS is marked in the top right panel as dark gray and gold dashed polygons, respectively. All spectroscopic sources are color-coded by redshift as indicated by the color bar.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: Left: smoothed density map of LAE candidates at z = 2.47. Red circles and salmon triangles represent pLAEs and sLAEs, respectively. The contours and background gray scale show the surface density levels relative to the field, and the red highlighted contour (﹩2.0\bar{{\rm{\Sigma }}}﹩) marks the threshold for protocluster selection. The yellow thick polygon shows the field of view of the HPS survey. The white dashed rectangle shows the field of view of the CLAMATO survey. Right: smoothed density map constructed by pLAEs only.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: NB422 − g color as a function of NB422 magnitude. All NB422 sources are represented by the gray scale and the contour lines. Photometric LAE candidates (pLAEs) selected using Equations (1) and (3) are shown as circles; triangles indicate the z fig3 = 2.40–2.52 sources satisfying the same criteria with a modified line excess Σ s  > 1 (sLAEs). The solid, dashed, and dashed–dotted curves show the Σ s  = 2 lines computed for the cosmosW, cosmosE, and cosmosC subfields, respectively. The horizontal dashed line marks the color corresponding to a rest-frame equivalent width W 0 = 50 Å at z = 2.45.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: The spectroscopic redshift distribution of the 70 LAEs with spectroscopic counterparts in the redshift range is shown. The red curve shows the NB422 filter transmission with arbitrary normalization. The inset shows the zoomed-out distribution including 5 low-z redshift interlopers. The red hatched bars highlight those at Hyperion redshift.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: Left: total throughput data (including filter transmission, mirror, optics, CCD quantum efficiency) of the filters listed in Table 1. Right: closeup view of NB422 where Lyα redshift is indicated on the top axis. Vertical lines mark the redshifts of the individual protoclusters in the survey field.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: Left: smoothed density map of LAE candidates at z = 2.47. The contours and background gray scale are identical to the left panel of Figure 4. The yellow thick polygon shows the field of view of the HPS survey. The white dashed rectangle shows the field of view of the CLAMATO survey. Right: smoothed density map using selected photometric galaxies in the COSMOS2015 catalog (Laigle et al. 2016).
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: A direct comparison of profiles of the stronger emission lines during post-outburst decline that shows the shapes and widths of the different types of lines. The profiles are normalized so the flat peaks of the broad components have the same flux. The forbidden lines and the Balmer and He I lines have very similar widths.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Deconvolution of the narrow and broad components of the stronger permitted and forbidden emission lines in the 2018 March 23 spectrum. The broad component can be fitted adequately with a trapezoid, whereas the narrow component, whose profile is influenced by blueward absorption, is approximately Gaussian.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: The BH accretion rates for different configurations distinguished by color. The same initial magnetic field B = 0.00033 is used for all simulated cases. The applied uniform magnetic field is normalized to the value of β. Here “inner” stands for the single torus case (see Figure 3), “outer” stands for the single outer torus case, “two-weak” stands for the case of the double torus configuration with a small outer torus (Figure 5), “two-strong” stands for the case of the double torus configuration with a huge outer torus (Figure 6), “two-corot” stands for the case of double corotating tori (Figure 7), and “two-contra” stands for the case of double counterrotating torus (Figure 9) simulations. All quantities here have geometrical units. Note that the accretion rate is normalized with the (same) central density of the inner torus for all cases (see Figure 4).
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Same as Figure 7 but for double tori rotating in opposite directions (“two-contra”). Color intensity corresponds to the values of the normalized mass density; blue (red) has been used for the positive (negative) angular momenta ℓ > 0 (ℓ < 0).
Paper: Effect of Dark Matter Distribution on Scalaron Gravity near the Galactic Center Black Hole and Its Prospects
Authors: P. C Lalremruati, Sanjeev Kalita
Figure caption: Variation of relative scalaron field amplitude with scalaron mass for different spins of the black hole. These variations are shown for the exponential dark matter profile having parameters displayed in the inset of the panels.
Paper: Effect of Dark Matter Distribution on Scalaron Gravity near the Galactic Center Black Hole and Its Prospects
Authors: P. C Lalremruati, Sanjeev Kalita
Figure caption: Variation of relative scalaron field amplitude with scalaron mass for different spins of the black hole. These variations are shown for the power-law dark matter profile, with parameters displayed in the inset of the panels.
Paper: Effect of Dark Matter Distribution on Scalaron Gravity near the Galactic Center Black Hole and Its Prospects
Authors: P. C Lalremruati, Sanjeev Kalita
Figure caption: The three-dimensional plots of the relative scalaron field amplitude (ψ 0/ϕ) with respect to the PPN parameters constrained near the Galactic Center black hole. The axis for ψ 0/ϕ in panel (f) is in the unit of 106 and that in panel (g) is in the unit of 10−19.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Same as Figure 4 but for IQ Tau. Note how the emitting radius (R  e ) is unconstrained for this source.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Same as Figure 4 but for BP Tau.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: Conditional H I mass function. The orange and green open circles represent the CHIMFs of satellites and centrals respectively. The black solid lines represent the CHIMFs of all galaxies. For comparison, the CHIMF of all galaxies in halos of ﹩\mathrm{log}{M}_{{\rm{h}}}\in [13.4,13.7)﹩ is plotted as the black dashed line in each panel. The red and blue solid lines are the CHIMFs of red and blue galaxies. The fitting result of central galaxies is shown as red and blue dashed lines for red and blue central galaxies. The colored numbers in each panel show the contribution of central (green), satellite (orange), red (red), and blue (blue) galaxies to the total H I mass, calculated using corresponding CHIMFs above M H I > 108 M ⊙. The gray-shaded region shows the H I mass range where the CHIMFs suffer from incompleteness.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: The H I mass function of galaxies. Left panel: the H I mass function of all galaxies in the local universe. The green open circles with errorbars are the results of this work using ﹩1/{V}_{\max }﹩ weighting method. The green dashed line is the fit to the green circles. The dark shaded region shows the HIMF derived from our luminosity function. The thick dark dashed line is the HIMF derived from conditional luminosity function (see Section 5.2). The magenta dashed line and open circles are the results of ALFALFA and xGASS (see Section 3.2). The gray-shaded region indicates the H I mass regime where SampleS is incomplete, and so the HIMF (green symbols) can only be considered as lower limits of the true HIMF. Right panel: the H I mass function of red and blue galaxies. The open circles are derived from ﹩1/{V}_{\max }﹩ method. The colored areas are derived from luminosity function. The solid lines are derived from conditional luminosity function.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: Probability distribution of model parameters. Contours correspond to 1σ and 2σ from inside out. The blue contours show the distribution of P( θ ∣ D ), and the red contours show the distribution of P( θ ∣ΦH I,  D ).
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: H I mass fraction as a function of galaxy properties for ALFALFA (top) /xGASS (bottom) mock and real survey. From left to right, the horizontal axis represents galaxy surface mass density, u − r color index, stellar mass, and galaxy concentration respectively. The y-axis is the observed H I mass fraction for H I-detected galaxies in real surveys and the estimated H I mass fraction for galaxies in mock surveys. The gray contours represent the volume-limited sample used in the mock ALFALFA survey. The contours include 5%, 15%, 25%, ..., 95% of the total sample. Galaxies outside these contours are shown as gray dots. The boxes show the 25%–75% percentile range of galaxies detected in mock surveys (magenta) or real surveys (cyan) in each bin. The vertical error bars show the 5%–95% percentile range. The green boxes show the distribution of the total xGASS sample (SampleX, detections + nondetections).
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: The distribution of our galaxy samples in NUV-r color and stellar mass diagram. Blue points are H I-detected galaxies in SampleX, and red crosses indicate H I nondetections in SampleX. Cyan contours indicate the distribution of SampleA galaxies. From inside to outside, the contours include 16%, 50%, and 84% of the SampleA respectively. The gray 2D histogram and dots show the distribution of SampleS galaxies.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: Normalized distribution of u − r, ﹩\mathrm{log}{M}_{* }﹩, and ﹩\mathrm{log}{M}_{{\rm{H}}\,{\rm\small{I}}}﹩ of galaxies. The cyan histogram represents the results of real samples, and the magenta histogram of mock samples. Both the gray solid histogram in the top panel and the gray dashed histogram in the bottom panel represent the SDSS volume-limited sample used to construct ALFALFA mock catalog. The gray solid histogram in the bottom panel represents the mean distribution of the 25 mock xGASS samples. The magenta-shaded area shows the 1σ scatter of the 25 mocks.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: The HIMF of ALFALFA and xGASS survey. The magenta points with errorbar are the ALFALFA 100% HIMF data points (Jones et al. 2018a). The magenta dashed line is the best fit to the data. The black open circle with errorbar is the xGASS HIMF derived in this work (see Section 2.3).
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: (a) Left: Cumulative distribution function (CDF) of the relative plane-of-sky angle between the magnetic field and outflow orientations, θ B−out, for the 200 protostellar outflow sources in the four cloud regions. The CDF expected from a random distribution of relative angles is also shown. (b) Right: CDF of θ B−out for all the outflows overlaid with the resampling test results from a uniform distribution (see text). Two blue lines indicate the upper and lower limits of the CDF when drawing 200 samples from a uniform distribution. The blue color scale illustrates the probability of a CDF drawn from a uniform distribution. The yellow line shows the results from Yen et al. (2021). The purple line shows the CDF of θ B−out, for the 136 highest-confidence protostellar outflow sources as discussed in Section 2.1.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption:  12CO (1 − 0) integrated intensity of Ophiuchus overlaid with the magnetic field streamlines derived from the Planck dust emission. Blue and red contours indicate the outflow lobes. Yellow lines indicate the orientation of the outflow lobe pairs.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Same as Figure 1, but for Orion.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Cumulative distribution functions (CDFs) of θ B−out in mock samples. Left: θ B−out distribution of the mock samples with different measurement uncertainties. The uncertainty is the total uncertainty, i.e., that of difference between their orientations on the pane of sky. Middle: θ B−out distribution of the mock samples with different 3D orientation angle distributions. Right: θ B−out distribution with different measurement uncertainties and different 3D orientation angle distributions.